Kavli Affiliate: Robert Cameron
| First 5 Authors: Akash Biswas, Bidya Binay Karak, Robert Cameron, ,
| Summary:
A striking feature of the solar cycle is that at the beginning, sunspots
appear around mid-latitudes, and over time the latitudes of emergences migrate
towards the equator.The maximum level of activity (e.g., sunspot number) varies
from cycle to cycle.For strong cycles, the activity begins early and at higher
latitudes with wider sunspot distributions than for weak cycles. The activity
and the width of sunspot belts increase rapidly and begin to decline when the
belts are still at high latitudes. Surprisingly, it has been reported that in
the late stages of the cycle the level of activity (sunspot number) as well as
the widths and centers of the butterfly wings all have the same statistical
properties independent of how strong the cycle was during its rise and maximum
phases.We have modeled these features using a Babcock–Leighton type dynamo
model and show that the flux loss through magnetic buoyancy is an essential
nonlinearity in the solar dynamo.Our study shows that the nonlinearity is
effective if the flux emergence becomes efficient at the mean-field strength of
the order of $10^4$~G in the lower part of the convection zone.
| Search Query: ArXiv Query: search_query=au:”Robert Cameron”&id_list=&start=0&max_results=10